DARTS/Astro Query System - SQL Search -

All the tables available for SQL Search and information on each table are listed in the Available Data page. Please see the User Guide for the usage of "SQL Search".

total 1

No.
object_name
center_ra
center_dec
center_ra_b1950
center_dec_b1950
center_ecliptic_lon
center_ecliptic_lat
center_galactic_lon
center_galactic_lat
roll_angle
observation_start_time_mjd
observation_start_time
observation_end_time_mjd
observation_end_time
observation_id
exposure
awarded_exposure
xis0_exposure
xis1_exposure
xis2_exposure
xis3_exposure
xis0_observation_mode
xis1_observation_mode
xis2_observation_mode
xis3_observation_mode
hxd_observation_mode
hxd_coarse_clock_rate_exposure
hxd_first_clock_rate_exposure
hxd_normal_clock_rate_exposure
hxd_all_clock_rate_exposure
hxd_wam_exposure
quantity_of_hxd_burst
processing_status
processing_date_mjd
processing_date
public_date_mjd
public_date
distribution_date_mjd
distribution_date
processing_version
processing_count
processing_software
proposal_id
proposal_abstract
proposal_category
proposal_category_code
proposal_priority
pi_name
co_pi_name
proposal_affiliated_country
proposal_cycle
observation_type
proposal_title
main_instrument
has_xis_injection
data_access_url
ql_access_url
ql_image_url
1 ETA CARINAE 161.1825 -59.711 160.696763 -59.447791 202.133764 -58.970475 287.57247158 -0.67238651 329.3001 56476.1821296296 2013-07-03 04:22:16 56479.0417361111 2013-07-06 01:00:06 408018010 97.524 180 97.524 97.524 0 97.524 2 2 0 2 1 0 0 87.8367 87.8367 247.0497 2 PROCESSED 57611.768912037 2016-08-11 18:27:14 56861 2014-07-23 00:00:00 56492.7286921296 2013-07-19 17:29:19 3.0.22.44 2 Hea_08Feb2016_V6.18_Suzaku_14Nov2013_V22 080081 Eta Carinae is a binary system containing two very massive main sequence stars orbiting with a period of 5.5 years. As reported by Sekiguchi et al. 2009 and Reitberger et al. 2012 based on Suzaku and Fermi data respectively, the system shows intense non-thermal emission extending from 20 keV to 200 GeV. Although detailed mechanism of this non-thermal emission has been clarified yet, it is now obvious that electrons and highly probably protons are accelerated to high energies by the collision of stellar winds. The aim of the present observation is to measure the spectral shape and flux of the non-thermal hard X-ray tail with the HXD, and compare with previous Suzaku observations. Based on a time variability (or non-variability), we examine proposed acceleration and emission mechanisms. GALACTIC POINT SOURCES 4 B TAKAYUKI YUASA JAP 8 AO8 DETAILED SPECTROSCOPY OF NON-THERMAL HARD X-RAY EMISSION OF ETA CARINAE HXD Y https://data.darts.isas.jaxa.jp/pub/suzaku/ver3.0/408018010/ Quick Look

Used SQL

SELECT * FROM suzaku_master_data WHERE observation_id = '408018010'

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